Beta Pic b, with an estimated mass of 11 times that of Jupiter, completes an orbit every 23 years at a distance of roughly 10 astronomical units (au). Previous observations using the original GRAVITY instrument suggested a low ratio of carbon isotopes—^12CO to ^13CO—in the planet’s atmosphere, hinting that it might have formed beyond the CO snowline where carbon monoxide exists mostly as ice. This scenario implied that the planet potentially migrated inward to its current position within the warmer inner disc, where CO should predominantly be gaseous.

However, the latest data acquired with GRAVITY+, which features upgraded adaptive optics and improved stability, paint a different picture. The team reports a significantly higher ^12CO/^13CO abundance ratio, one that aligns well with isotopic ratios found in the Solar System and the broader interstellar medium. This finding places Beta Pic b’s origin inside the CO snowline, consistent with its current orbit and challenging previous assumptions about large planetary migrations in this system.

The detection of ^13CO required sophisticated analysis due to its faint signal, but its measurement alongside ^12CO underscores GRAVITY+’s extraordinary data quality. In addition to composition, the team observed subtle photometric variations likely linked to Beta Pic b’s rotation period of approximately 8.7 hours, hinting at dynamic atmospheric phenomena such as cloud patterns or chemical weather. While these variations need confirmation through more sensitive follow-up studies, they mark a fascinating glimpse into the atmospheric complexity of a young exoplanet.

Despite these advances, the study raises questions about the utility of carbon isotope ratios as clear tracers of planetary birthplaces. The homogeneity of measured ^12CO/^13CO ratios among numerous young gas giants suggests that the ratio may not reliably differentiate between formation zones inside or outside the snowline. Scientists suspect that current models of CO ice chemistry in protoplanetary discs lack crucial physics, preventing precise interpretation of isotope data as indicators of planetary origins.

This insight underscores the complexity of planet formation and the challenges inherent in decoding the histories of distant worlds. Nevertheless, GRAVITY+ stands out as a powerful instrument poised to revolutionize exoplanet characterization with its unparalleled precision. As researchers continue refining observational techniques and theoretical models, tools like GRAVITY+ are likely to unlock new avenues for understanding giant planet formation and atmospheric dynamics in young planetary systems.

The study exemplifies a step forward in planetary science, showing how cutting-edge instrumentation can refine and sometimes overturn prevailing interpretations. Beta Pictoris b remains a tantalizing laboratory for investigating the processes that shape planetary systems, and with continued observations, astronomers move closer to unraveling the complex interplay of chemistry, dynamics, and formation history written in exoplanet atmospheres.

Subject of Research: Not applicable
Article Title: 13CO and potential variability in β Pictoris b with GRAVITY+
News Publication Date: 9-Jul-2026
Web References: DOI: 10.1051/0004-6361/202660275
Image Credits: ESO/L. Calçada
Keywords: Beta Pictoris b, exoplanets, planet formation, circumstellar discs, carbon isotopes, GRAVITY+, Very Large Telescope Interferometer, atmospheric variability

Hot Jupiters are a fascinating class of exoplanets typified by their colossal size—often comparable to or exceeding that of Jupiter—and their blisteringly close orbits around host stars, sometimes completing a single revolution in mere days. Because of these properties, hot Jupiters serve as prime candidates for detailed atmospheric studies. Their proximity to the parent star means they receive intense irradiation, significantly influencing their atmospheric dynamics, radiative properties, and chemical compositions. This environment makes them critical laboratories for testing and refining planetary formation, evolution, and climate models.

The accepted paradigm for hot Jupiter atmospheres is predicated on tidal locking, whereby the planet’s rotation period synchronizes with its orbit, causing one hemisphere to perpetually face the star, exposed to relentless stellar radiation, while the opposite side remains cloaked in darkness. This lock is thought to occur rapidly due to strong gravitational interactions between the planet and its star. The perpetual dayside is expected to feature a dominant hot spot slightly offset towards the direction of planetary rotation and orbital motion, driven by atmospheric super-rotation. This consistent pattern is observed across many studied hot Jupiters, reinforcing tidal locking as a foundational concept within exoplanetary atmospheric science.

However, CoRoT-2 b stands out starkly against this backdrop. Discovered in 2007 and studied extensively since, this hot Jupiter’s hottest atmospheric region is displaced not ahead of but behind the substellar point—the point on the planet directly facing its star—opposite to the behavior seen in counterparts. Initial hypotheses proposed to explain this anomaly included obscuring cloud layers, magnetic field-driven atmospheric dynamics complicating wind patterns, or a rotation period differing from the orbital period. Previous work by Lisa Dang, a collaborator and professor at the University of Waterloo, outlined these potential explanations based on early observational data.

Aurora Kesseli and her team recently applied phase-resolved emission spectroscopy using the CRIRES+ instrument on the VLT, capturing the planet’s atmosphere in unprecedented detail across different orbital phases. This method enables tracing variations in emitted light corresponding to temperature and wind structures dynamically as the planet orbits. The data conclusively pointed toward the third hypothesis: CoRoT-2 b exhibits a rotation rate slower than its orbital period, meaning it is not synchronized tidally. Specifically, one full rotation of CoRoT-2 b lasts approximately three Earth days, while its orbital period is about 1.5 days. This differential implies that by the time the planet completes a single axial spin, it has circumnavigated its host star twice.

This non-synchronous rotation leads to a decoupling of the traditional tidally locked pattern of day-night heating contrasts, fundamentally altering how atmospheric circulation redistributes energy. Without tidal locking, the expected eastward-shifted hot spot is replaced by a distinct thermal signature resulting from slower planetary spin interacting with intense stellar irradiation. The discovery challenges standard assumptions embedded in many exoplanet climate models that universally prescribe tidal locking for hot Jupiters, suggesting a more nuanced picture with rotational diversity.

Understanding the rotational state of exoplanets like CoRoT-2 b carries broader implications, especially in the context of habitability studies. Many terrestrial exoplanets orbit M dwarfs, cool stars constituting roughly 70% of the stellar population in the Milky Way. These stars have habitable zones—regions where liquid water can persist on planetary surfaces—so close that tidal locking is highly probable within relatively short stellar lifetimes. Since rotation influences temperature gradients, weather systems, and atmospheric retention, a tidally locked terrestrial exoplanet’s climate could differ drastically from one with asynchronous rotation. Hence, unraveling CoRoT-2 b’s rotation contributes to refining the models employed for predicting environments on potentially habitable worlds in tight orbits.

While the revelation of CoRoT-2 b’s slow rotation solves a significant piece of the puzzle, it simultaneously opens further questions. The mechanisms driving this atypical rotational state in a planet where tidal forces should dominate remain elusive. Possible contributors might include magnetic torques, differential interior structures, or recent dynamical interactions within its planetary system that disturbed its spin. Future observations, especially with upcoming flagship observatories like the James Webb Space Telescope, the Habitable Worlds Observatory, and the ground-based Extremely Large Telescope, promise to provide deeper insight into these processes by offering higher precision data across broader wavelength ranges.

Hot Jupiters continue to act as vanguards in exoplanetary science. They are currently the best-understood and most accessible class of exoplanets for atmospheric characterization, enabling astronomers to test and recalibrate models of atmospheric physics, chemistry, and dynamics. The case of CoRoT-2 b exemplifies how nature’s variability often defies simplified expectations, compelling constant refinement of theories and models. These advances do not merely enhance comprehension of gas giants but ripple outward to shape understanding of all planetary atmospheres, including those bearing life.

Kesseli underscores the excitement of probing “weird” exceptions within the exoplanet census, emphasizing that such outliers drive scientific progress. As instrumentation improves and more extensive surveys unfold, the taxonomy of exoplanetary rotation states, atmospheric dynamics, and climate regimes will grow richer. This improved framework will essentialize our broader quest to understand planet formation, stellar influences, and potential biosignatures on distant worlds. CoRoT-2 b’s defiance of tidal locking invites the scientific community to remain alert to unexpected phenomena lurking in exoplanet atmospheres.

In summation, the unraveling of CoRoT-2 b’s anomalous atmospheric hot spot through rigorous spectroscopic measurements marks a milestone in exoplanet research. It dispels the notion of universal tidal locking among hot Jupiters and reveals a more intricate rotational behavior impacting atmospheric properties. The ongoing inquiry into the cause of this slowed rotation will propel future efforts to decipher planetary spins, magnetic interactions, and orbital dynamics across a diverse planetary population. These insights will deepen our grasp of planetary physics and help guide the search for habitable environments beyond our solar system.

Subject of Research: Atmospheric dynamics and rotational state of the hot Jupiter CoRoT-2 b
Article Title: Unraveling the Mystery of the Peculiar and Young Hot Jupiter CoRoT-2b II: Phase Resolved Emission Spectroscopy with VLT/CRIRES+ and Gemini-S/IGRINS
News Publication Date: June 16, 2026
Web References: IPAC News, NExScI at Caltech, University of Waterloo Newsroom
References: Kesseli et al., submitted to The Astronomical Journal
Image Credits: Keith Miller (Caltech/IPAC – SELab)

Keywords: hot Jupiter, CoRoT-2 b, tidal locking, exoplanet atmospheres, phase-resolved spectroscopy, planetary rotation, atmospheric dynamics, VLT/CRIRES+, exoplanet climate models, M dwarf habitability, rotational decoupling, spectroscopic observations

Unlike the familiar gas giants of our solar system such as Jupiter and Saturn, which orbit far from the sun and feature frigid environments, TOI-199b exists in a temperate regime rarely observed among exoplanets. This positions it between the extremely cold gas giants we know and the scorching “hot Jupiters” whose orbits bring them perilously close to their stars. Its moderate temperature, measured at about 175 degrees Fahrenheit, represents an intriguing middle ground, offering a closer analogue to planetary conditions that might be more common across the galaxy.

The team, led by scientists at Penn State University and NASA’s Jet Propulsion Laboratory (JPL), employed a method known as transmission spectroscopy to unravel the secrets of TOI-199b’s atmosphere. This technique hinges on analyzing starlight that filters through an exoplanet’s atmosphere as it transits—or passes in front of—its host star. As the stellar light traverses gaseous layers enveloping the planet, molecules within absorb specific wavelengths, imprinting a spectral signature that can be decoded by telescopic instruments.

What sets the JWST apart in this endeavor is its unparalleled sensitivity and spectral resolution, enabling the detection of subtle atmospheric fingerprints that previous observatories could not discern. Over about 20 hours of consecutive observations, followed by a seven-hour transit event, the scientists dissected the star’s light into its constituent colors. This allowed them to identify the characteristic absorption bands of methane unequivocally, confirming longstanding theoretical predictions about the chemistry of temperate gas giants.

The planetary orbit of TOI-199b, with a period close to one hundred Earth days, ensures conditions conducive to both observation and habitability comparative studies. Although its surface temperatures are too high to sustain Earth-like life, the discovery provides an essential benchmark for understanding atmospheric processes on gaseous planets orbiting at comfortable distances from their stars. The atmospheric methane signature not only affirms models developed to explain such exoplanets but also offers insights into carbon chemistry and dynamics that might influence Earth’s own atmospheric evolution.

Interestingly, the initial spectroscopic data also hinted at the presence of other molecules such as ammonia and carbon dioxide. These tentative findings could signal complex atmospheric interactions, possibly analogous to those on the gas giants in our own solar neighborhood. Future observations, utilizing targeted spectroscopic campaigns, aim to quantify the abundances of these gases with greater precision, deepening our comprehension of the planet’s climate and chemistry.

The significance of studying temperate gas giants like TOI-199b transcends mere cataloging of exoplanet types; it directly informs broader theories about planetary formation and atmospheric evolution. By comparing diverse planetary atmospheres across different systems, astronomers seek to decipher the physical and chemical processes that shape worlds. Such research may eventually illuminate the conditions that foster habitability, as well as the evolutionary pathways that planets, including Earth, have undergone.

The technical execution of this study exemplifies how JWST’s state-of-the-art instruments revolutionize exoplanetary science. The telescope’s ability to perform high-precision spectroscopic monitoring over extended periods was crucial, particularly given the comparatively long transit duration of TOI-199b’s orbit. This contrasts with shorter transits typical of hot Jupiters, which last less than an hour, thereby offering less observational data and increasing the challenge of atmospheric characterization.

By pioneering the first detailed atmospheric analysis of a temperate gas giant, this research opens the door to more expansive surveys of similar exoplanets. The uniqueness of TOI-199b has raised compelling questions: Is this methane-rich atmosphere a universal trait among such temperate giants, or an outlier shaped by peculiar local factors? Equipped with JWST and complementary space and ground-based facilities, astronomers are poised to answer these questions in the coming years.

The international team behind this breakthrough includes experts from Penn State, JPL, Arizona State University, Johns Hopkins University, the Carnegie Institution for Science, Caltech, and the University of California Santa Cruz. Their collaborative effort underscores the interdisciplinary and global nature of modern astronomical research, combining theoretical models, observational technology, and analytical expertise to push the frontier of exoplanetary knowledge.

Ultimately, this discovery underscores the transformative potential of cutting-edge space telescopes like JWST to unlock the mysteries of distant worlds, not just blazing hot gas giants but also those with more temperate environments. By advancing our understanding of atmospheric chemistry and planetary climates far beyond our solar system, we inch closer to answering fundamental questions about the universe, including the nature of planets where life might exist or could arise in the future.

Subject of Research: Not applicable
Article Title: Methane on the Temperate Exo-Saturn TOI-199b
News Publication Date: 20-May-2026
Web References: https://doi.org/10.3847/1538-3881/ae4fba
References: Astronomical Journal, Vol. [specific volume and issue unavailable], DOI: 10.3847/1538-3881/ae4fba
Image Credits: NASA/JPL-Caltech

Keywords

exoplanet, TOI-199b, methane, James Webb Space Telescope, JWST, transmission spectroscopy, temperate gas giant, atmospheric composition, planetary formation, atmospheric evolution, methane detection, astronomy

Unlike Earth, which formed with relatively thin hydrogen-poor atmospheres, these exotic planets possess envelopes rich in molecular hydrogen (H₂) that press upon molten rocky mantles under colossal pressures and temperatures. Theoretical models have long postulated that such an environment fosters chemical reactions between hydrogen gas and the underlying silicate magma, producing water that could profoundly alter the planet’s internal chemistry and atmospheric characteristics. However, these models have suffered from a dearth of direct experimental evidence, largely due to the immense technological challenges of recreating such extreme conditions in a laboratory setting.

Addressing this critical gap, an international team of researchers led by Miozzi, Shahar, and Young has conducted cutting-edge experiments using laser-heated diamond anvil cells to replicate the intense pressures ranging from 16 to 60 gigapascals (GPa) and temperatures exceeding 4000 Kelvin typical of magma ocean conditions in sub-Neptune interiors. These experiments are among the few to reach such extreme thermodynamic regimes while simultaneously probing the chemical interactions between molecular hydrogen and silicate melts, which are highly representative of planetary interiors.

The experimental results paint a remarkable picture: hydrogen, far from being chemically inert under these extreme conditions, dissolves copiously into silicate melts, with the degree of dissolution strongly influenced by temperature rather than pressure. As temperature rises, the solubility of hydrogen in the molten silicate increases significantly, indicating that hotter planetary interiors could promote more intense chemical exchange between atmosphere and magma than previously thought. This temperature-dependent solubility overturns prior assumptions that pressure would be the dominant factor controlling hydrogen incorporation.

In tandem with hydrogen dissolution, the experiments reveal a thermochemical transformation of iron-bearing components within the melt. Specifically, iron oxide (FeO), a common constituent of silicate minerals, undergoes reduction in the presence of molecular hydrogen. This reduction yields substantial quantities of water through the formation of hydroxyl groups in the silicate matrix, accompanied by the segregation of iron-rich metallic blebs. This process effectively converts atmospheric hydrogen and iron oxides into water and metallic iron, a reaction that was previously hypothesized but never empirically demonstrated at such extreme planetary conditions.

The implications of these findings ripple across several domains of planetary science. Foremost, they suggest that the typical accretion and differentiation processes during planet formation naturally generate significant amounts of water deep within planetary interiors, even in environments initially rich in hydrogen gas but poor in free oxygen. This in situ water production challenges the traditional view of water delivery solely via volatile-rich planetesimals or external cometary bombardment, positioning hydrogen-magma reactions as a central mechanism in early planetary water budgets.

Moreover, the generation of water in the deep magma ocean may influence the viscosity, melting behavior, and convective dynamics of planetary mantles. Water acts as a potent flux in silicate melts, lowering melting temperatures and facilitating differentiation, potentially shaping the evolution of magnetic fields, tectonics, and atmosphere-interior exchanges in sub-Neptune planets. The formation of iron-enriched metallic droplets could also contribute to the development of layered interiors or core formation pathways distinct from those on Earth.

From an atmospheric perspective, the findings imply that substantial water vapor could outgas from the magma ocean into the overlying hydrogen atmosphere, altering its chemical composition and spectral signatures. This could impact the detectability and characterization of exoplanet atmospheres through telescopes and space missions, providing new markers for the presence of internal magmatic activity and water generation.

Crucially, this experimental breakthrough bridges a fundamental knowledge gap between geochemistry, planetary physics, and exoplanetary atmospheric science. For the first time, robust laboratory measurements underpin hypotheses on hydrogen-silicate melt interactions, allowing modelers to refine simulations of planet formation, interior evolution, and volatile cycling on worlds vastly different from Earth. The work also opens paths for future experiments at even more extreme conditions or with varied starting compositions to explore the generality of these reactions.

The methodology employed—laser heating within a diamond anvil cell—represents the forefront of high-pressure experimental technology. By focusing an intense laser beam onto a tiny sample chamber compressed between two diamond anvils, temperatures above 4000 K are achieved while maintaining static pressures up to 60 GPa. This capability is essential to mimic the conditions deep inside planets many times more massive than Earth, where the magma ocean and atmosphere interact. Precise in situ spectroscopic probes elucidate the chemistry and phase changes occurring during experimentation.

In sum, the experimental results from Miozzi and colleagues signify a paradigm shift in our understanding of how water, a key ingredient for habitability and planetary evolution, can arise internally from primordial hydrogen atmospheres and magma oceans. Rather than requiring external sources, significant water inventories may be generated intrinsically through elemental reduction mechanisms at extreme conditions. This fundamentally alters conceptions of planetary volatile reservoirs and suggests a ubiquitous process that could operate throughout the Galaxy on countless rocky worlds with thick hydrogen envelopes.

As exploration of exoplanetary systems advances, integrating such high-pressure geochemical insights becomes indispensable for interpreting observational data and assessing the potential for habitable environments beyond Earth. This research stands as a milestone that unifies experimental petrology with exoplanet science, shedding light on the nature of worlds that, until recently, existed only in models and theoretical imaginations.

The future of planetary science lies in these interdisciplinary endeavors, where physics, chemistry, and astronomy converge to unravel the complex histories of distant planets. The newly revealed extreme generation of water during planet formation reinforces that the Universe’s capacity to produce diverse planetary outcomes is even more remarkable than imagined. With these findings, we take a crucial step closer to comprehending the diversity and complexity of planets orbiting other stars and the many ways in which the basic ingredients for life may assemble across cosmic time.

Subject of Research:
High-pressure experimental investigation of hydrogen-silicate melt interaction and water generation during planet formation.

Article Title:
Experiments reveal extreme water generation during planet formation.

Article References:
Miozzi, F., Shahar, A., Young, E.D. et al. Experiments reveal extreme water generation during planet formation. Nature (2025). https://doi.org/10.1038/s41586-025-09816-z

Image Credits: AI Generated

WASP-121b is a striking example of an ultra-hot Jupiter, orbiting so close to its star that its orbital radius is roughly double the stellar diameter. Completing a rotation in just over 30 hours, the planet presents a dichotomy of hemispheres: a blisteringly hot dayside where temperatures soar beyond 3000°C and a comparatively cooler nightside that lingers near 1500°C. These extreme thermal gradients drive complex atmospheric dynamics and chemistry, culminating in a uniquely stratified atmospheric environment that challenges existing theoretical models of exoplanet atmospheres.

Central to this study is the identification of silicon monoxide (SiO) gas in WASP-121b’s atmosphere. Silicon, initially sequestered in solid form within rocky materials like quartz housed in planetesimals, only entered the gaseous envelope during the later stages of the planet’s formation. This crucial observation indicates that WASP-121b’s accretion of rocky solids unfolded concurrently with, or just after, the majority of its atmospheric gas accumulation—a revelation that nuances our understanding of how refractory elements become incorporated into gas giant atmospheres.

The researchers leveraged the JWST’s Near-Infrared Spectrograph (NIRSpec) to monitor WASP-121b across its orbit, capturing the planet’s emergent emission spectra as different portions of its atmosphere rotated into view. This temporal resolution allowed them to dissect spatial variations in atmospheric chemistry between day and night hemispheres. Additionally, transit spectroscopy provided a glimpse into the composition of the atmospheric limb, where dayside and nightside flows intertwine, offering a holistic view of the planet’s atmospheric structure.

One of the more surprising outcomes of the observations was the prominent detection of methane (CH₄) on the cooler nightside, contradicting models that predict its rapid depletion in ultra-hot atmospheres. Methane’s molecular instability at extreme dayside temperatures leads to its expected scarcity, yet its abundance on the nightside implies complex vertical and horizontal atmospheric dynamics. The team posits that robust vertical mixing currents transport methane-rich gas from lower atmospheric layers upward to replenish the depleted upper atmosphere, indicating vigorous vertical winds previously unaccounted for in exoplanet atmospheric models.

The chemical inventory drawn from these observations reveals a super-stellar carbon-to-oxygen (C/O) ratio in WASP-121b’s atmosphere, a signature pointing to its formation in a cold, methane-rich region of its protoplanetary disk. This region would have been warm enough for methane to exist in gaseous form, yet cold enough to lock water ice in solid pebbles that did not accrete onto the planet. Such selective accumulation enriched the planet’s gas envelope with carbon while simultaneously biasing the atmosphere toward lower oxygen content.

This scenario implies WASP-121b formed beyond the water ice line—akin to an orbital distance between Jupiter and Uranus in our own Solar System—before migrating inward to its current perilously close orbit. The inward spiral would have involved traversing the protoplanetary disk, perhaps via interactions with the disk’s gas and planetesimal populations, ultimately settling just outside its star, where intense stellar irradiation sculpts its current atmospherics.

The discovery of silicon monoxide serves as a proxy for the rock-forming materials delivered during formation, implying that solid planetesimals were still accreting during the latter gaseous envelope stage. This sustained accretion of silicate-bearing solids, amidst an environment enriched by carbonaceous gas, could explain the atmospheric composition now observed. It underscores a multiphase planetary assembly process, highlighting the importance of solid-gas interactions and migration in shaping exoplanet atmospheres.

Spectroscopic data from the transit – the passage of WASP-121b across its star’s disk – complements emission measurements by sampling atmospheric layers where dayside and nightside gases mingle. Intriguingly, methane was notably absent in this transitional limb region, reinforcing the idea that methane distribution is controlled by dynamic atmospheric flows and temperature gradients rather than being uniformly mixed around the planet.

These intricate findings challenge the prevailing assumptions in exoplanet atmospheric science, especially regarding vertical mixing and chemical kinetics. Existing atmospheric circulation models often approximate horizontal heat redistribution without fully accounting for powerful vertical currents. WASP-121b’s atmospheric profile suggests that incorporating vertical transport processes is essential for accurate portrayals of exoplanet atmospheres, particularly those subjected to extreme stellar irradiation.

The JWST’s instrumentation, particularly NIRSpec, was pivotal in enabling this deep characterization. By capturing spectra across multiple orbital phases and leveraging cutting-edge detector technology, these observations achieved unprecedented sensitivity and resolution, revealing subtle atmospheric molecules that had eluded previous missions. This underscores JWST’s monumental impact on exoplanetary science, transforming theoretical speculation into empirical understanding.

Beyond WASP-121b, the study sets a benchmark for the investigation of exoplanet atmospheres, providing a natural laboratory where the interplay of extreme irradiation, atmospheric chemistry, and planetary migration can be dissected in exquisite detail. The implications permeate planetary formation theory, atmospheric dynamics, and the wider understanding of chemical evolution in exoplanetary systems, paving the path for future explorations with JWST and beyond.

As telescopes like JWST continue to peer into the atmospheres of distant worlds, the story of WASP-121b exemplifies the complex and dynamic nature of planet formation and atmospheric evolution. It reveals a world where chemical fingerprints narrate a voyage from cold outer realms to blazing proximity with a star, unveiling the universal processes that sculpt planetary systems across the galaxy.

Subject of Research: Not specified in detail beyond exoplanet atmospheric composition and formation mechanisms.

Article Title: SiO and a super-stellar C/O ratio in the atmosphere of the giant exoplanet WASP-121b

News Publication Date: 2 June 2025

Web References: https://dx.doi.org/10.1038/s41550-025-02513-x

References: Study published in Nature Astronomy, 2025

Image Credits: T. Müller (MPIA/HdA)

Keywords

Exoplanet atmosphere, WASP-121b, methane, silicon monoxide, carbon-to-oxygen ratio, JWST, NIRSpec, ultra-hot Jupiter, planetary migration, protoplanetary disk, vertical atmospheric mixing, spectroscopic observation